IOTA: recent technology and science

Traub, W. A.; Berger, J.‐P.; Brewer, Michael K.; Carleton, N. P.; Kern, P.; Kraus, Stefan; Lacasse, M. G.; McGonagle, William H.; Millan-Gabet, R.; Monnier, John D.; Pedretti, E.; Ragland, Sam; Reich, R.; Schloerb, F. Peter; Schüller, Peter; Souccar, Kamal; Wallace, Gary

doi:10.1117/12.550916

Cited by 10 publications

(5 citation statements)

References 23 publications

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“…Application at higher frequencies was first mentioned by Rogstad (1968), but only much later carried out in the visible/IR through aperture masking experiments (Baldwin et al 1986, Haniff et al 1987, Readhead et al 1988, Haniff et al 1989. Currently three separate-element interferometers have succeeded in obtaining closure phase measurements in the visible/IR, first at COAST (Baldwin et al 1996), soon after at NPOI (Benson et al 1997), and most recently at IOTA (Traub 2003).…”

Section: Closure Phases Consider Figurementioning

confidence: 99%

Optical interferometry in astronomy

2003

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Abstract. Here I review the current state of the field of optical stellar interferometry, concentrating on ground-based work although a brief report of space interferometry missions is included. We pause both to reflect on decades of immense progress in the field as well as to prepare for a new generation of large interferometers just now being commissioned (most notably, the CHARA, Keck and VLT Interferometers). First, this review summarizes the basic principles behind stellar interferometry needed by the lay-physicist and general astronomer to understand the scientific potential as well as technical challenges of interferometry. Next, the basic design principles of practical interferometers are discussed, using the experience of past and existing facilities to illustrate important points. Here there is significant discussion of current trends in the field, including the new facilities under construction and advanced technologies being debuted. This decade has seen the influence of stellar interferometry extend beyond classical regimes of stellar diameters and binary orbits to new areas such as mapping the accretion disks around young stars, novel calibration of the Cepheid Period-Luminosity relation, and imaging of stellar surfaces. The third section is devoted to the major scientific results from interferometry, grouped into natural categories reflecting these current developments. Lastly, I consider the future of interferometry, highlighting the kinds of new science promised by the interferometers coming on-line in the next few years. I also discuss the longer-term future of optical interferometry, including the prospects for space interferometry and the possibilities of large-scale ground-based projects. Critical technological developments are still needed to make these projects attractive and affordable. †

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Section: Closure Phases Consider Figurementioning

confidence: 99%

Optical interferometry in astronomy

2003

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“…The 3 IOTA telescopes each have a diameter of 0.45 m, and a minimum-to-maximum baseline range of 5-38 m. The telescopes are movable among 17 stations, along 2 linear arms, within this range. IOTA achieved first fringes with two telescopes in December 1993, and more recently, IOTA has been upgraded with the addition of a third telescope and a new control system for the interferometer (Traub et al 2004). An aerial view of the IOTA 3-telescope interferometer is shown in Figure 1 (left).…”

Section: Instrumentationmentioning

confidence: 99%

Characterizing closure-phase measurements at IOTA

Ragland

Traub

Berger

et al. 2004

New Frontiers in Stellar Interferometry

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We are working towards imaging the surfaces and circumstellar envelopes of Mira stars in the near-infrared, using the IOTA interferometer and the IONIC integrated-optics 3-beam combiner. In order to study atmospheric structures of these stars, we installed 3 narrow-band filters that subdivide H-band into 3 roughly equal-width sub-bands-a central one for continuum, and 2 adjacent ones to sample Mira star's (mostly water) absorption-bands. We present here our characterization of the IOTA 3-Telescope interferometer for closure-phase measurements with broad and narrow-band filters in the H atmospheric window. This includes characterizing the stability, chromaticity, and polarization effects of the present IOTA optics with the IONIC beam-combiner, and characterizing the accuracy of our closure phase measurements.

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“…1 The first home of FLUOR, where it produced the first scientific results, was IOTA. 2 While the FLUOR/IOTA combination was extremely fruitful, the baselines of IOTA, which range from 5 to 30 meters, did not offer the large angular resolution, of the order of one milliarcsecond or less, required for some programs, especially Cepheids pulsating stars, debris disks or young stellar object. In 2002, FLUOR moved 3 from IOTA to the CHARA Array, 4,5 which offered larger baselines (from 33 to 330 meters) and larger collecting telescopes.…”

Section: Introductionmentioning

confidence: 98%